how do multiple planetary systems shape the
dust disk?
The HL Tau system
.
Giovanni Picogna
Tübingen Universität, CPT & Kepler Center
6th May 2015
Exoplanets in Lund 2015
Lund Observatory
.introduction
.
the hl tau system
∙ We are now obtaining pristine images of the protoplanetary disk
evolution that we can use to constraint planet formation models.
2
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the hl tau system
∙ We are now obtaining pristine images of the protoplanetary disk
evolution that we can use to constraint planet formation models.
∙ an outstandig example is the HL Tau system, imaged by ALMA in
the mm continuum
Figure 1:
HL Tau system. Source: http://www.eso.org/public/news/eso1436/
2
.
the hl tau system
∙ We are now obtaining pristine images of the protoplanetary disk
evolution that we can use to constraint planet formation models.
∙ an outstandig example is the HL Tau system, imaged by ALMA in
the mm continuum
∙ where axysimmetric ring structures and gaps are visible
Figure 1:
HL Tau system - continuum 233 GHz image. Source: http://www.eso.org/public/news/eso1436/
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ring structure formation
There are different physical processes capable of creating rings in a
disk:
∙ multi-planetary system
Figure 2: Meru et al., 2014
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ring structure formation
There are different physical processes capable of creating rings in a
disk:
∙ multi-planetary system
∙ zonal flows
Figure 2: Flock et al., 2014
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multi-planetary system scenario
I focus on the planetary origin of those structure
∙ straightforward explanation
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multi-planetary system scenario
I focus on the planetary origin of those structure
∙ straightforward explanation
∙ no detailed analysis yet of dust filtration and dynamical evolution
in a multi-planetary system
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.numerical method
.
numerical method
∙ I have used the FARGO 2D code (Masset et al., 2000)
Quantity
Cells in radial direction
Cells in azimuthal direction
Inner boundary
Outer boundary
Value
256
512
Open
Non–reflecting
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.
numerical method
∙ I have used the FARGO 2D code (Masset et al., 2000)
∙ modified to study the dynamic of a population of small bodies
treated as Lagrangian particles (Müller)
Quantity
Cells in radial direction
Cells in azimuthal direction
Inner boundary
Outer boundary
Value
256
512
Open
Non–reflecting
6
.
numerical method
∙ I have used the FARGO 2D code (Masset et al., 2000)
∙ modified to study the dynamic of a population of small bodies
treated as Lagrangian particles (Müller)
∙ integrated with a semi–implicit and fully implicit integrator in
cylindrical choordinates as in Zhu et al. (2014)
Quantity
Cells in radial direction
Cells in azimuthal direction
Inner boundary
Outer boundary
Value
256
512
Open
Non–reflecting
6
.
parameter space
Physical quantity
Disk mass (M⊙ )
Disk extent (au)
Aspect ratio
Viscosity (αSS )
Surface density profile
Temperature profile
EOS
Dust particles
Dust density (g/cm3 )
Dust size (cm)
Star mass (M⊙ )
Planet masses (Mth )
Planet semi–major axes (au)
Value
0.135
[2.5,100]
0.05
0.004
-1
-1
Isothermal
1 × 106
2.6
0.1,1,10,100
0.55
1,5,10
25,50
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limitations
∙ no self-gravity
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limitations
∙ no self-gravity
∙ no back reaction of the particles on the gas
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limitations
∙ no self-gravity
∙ no back reaction of the particles on the gas
∙ isothermal EOS
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limitations
∙ no self-gravity
∙ no back reaction of the particles on the gas
∙ isothermal EOS
∙ 2D simulations
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.major physical parameters
.
gap opening criteria
∙ Thermal criterion
Mth =
Mp
=q>
M⋆
( )3
cs 3
H
= M⋆
GΩp
R
( )3
H
= 1.25 × 10−4
R
∙ Viscous criterion
40ν
q≥ 2
= 40αSS
Rp Ω p
( )2
H
= 4 × 10−4
R
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stopping time
∙ It quantifies the coupling between the solid and gas components
∙ We adopted the formula by Haghighipour & Boss (2003) that
smoothly combines the Epstein and Stokes regimes.
τs = τf ΩK =
[
]−1
ρ• a•
3
(1 − f)vth + fCD vrel
ΩK
ρg
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1
FD = − ∆vp
τf
∙ For our parameters the dm-size particles have a stopping time ∼ 1
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.results
.
10 thermal masses
∙ mm cm dm m –sized particle evolution
For videos look at this webpage
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10 thermal masses
∙ ring fragmentation in 5 high–mass stable points near 5:3 orbital
resonance with the inner planet
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10 thermal masses
∙ ring fragmentation in 5 high–mass stable points near 5:3 orbital
resonance with the inner planet
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10 thermal masses
∙ ring fragmentation in 5 high–mass stable points near 5:3 orbital
resonance with the inner planet
∙ vortices formation in the inner gap
Figure 3: cm-sized particles
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10 thermal masses
∙ ring fragmentation in 5 high–mass stable points near 5:3 orbital
resonance with the inner planet
∙ vortices formation in the inner gap
∙ coorbital regions destabilized by the outer planet
Figure 3: cm-sized particles
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10 thermal masses
∙ ring fragmentation in 5 high–mass stable points near 5:3 orbital
resonance with the inner planet
∙ vortices formation in the inner gap
∙ coorbital regions destabilized by the outer planet
∙ mm-size dust migrate through the gap
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10 thermal masses
∙ Final surface density distribution
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10 thermal masses
∙ Final surface density distribution
∙ Final eccentricity distribution
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5 thermal masses
∙ mm cm dm m –sized particle evolution
For videos look at this webpage
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5 thermal masses
∙ ring fragmentation in 5 high–mass stable points
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5 thermal masses
∙ ring fragmentation in 5 high–mass stable points
∙ no long–lived vortex
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5 thermal masses
∙ ring fragmentation in 5 high–mass stable points
∙ no long–lived vortex
∙ coorbital regions destabilized by the outer planet
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5 thermal masses
∙ ring fragmentation in 5 high–mass stable points
∙ no long–lived vortex
∙ coorbital regions destabilized by the outer planet
∙ particle exchange between coorbital regions
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5 thermal masses
∙ Final surface density distribution
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5 thermal masses
∙ Final surface density distribution
∙ Final eccentricity distribution
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1 thermal mass
∙ mm cm dm m –sized particle evolution
For videos look at this webpage
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1 thermal mass
∙ Ripples in m-sized particles distribution
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1 thermal mass
∙ Ripples in m-sized particles distribution
∙ Particles in coorbital region very close to the planet location
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1 thermal mass
∙ Ripples in m-sized particles distribution
∙ Particles in coorbital region very close to the planet location
∙ Ring is wider and do not fragment
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1 thermal mass
∙ Final surface density distribution
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1 thermal mass
∙ Final surface density distribution
∙ Final eccentricity distribution
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what’s next?
∙ Generate ALMA–like images (e.g. with RADMC-3D + CASA package)
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what’s next?
∙ Generate ALMA–like images (e.g. with RADMC-3D + CASA package)
∙ Extend integration time
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what’s next?
∙ Generate ALMA–like images (e.g. with RADMC-3D + CASA package)
∙ Extend integration time
∙ Add particle back-reaction
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what’s next?
∙ Generate ALMA–like images (e.g. with RADMC-3D + CASA package)
∙ Extend integration time
∙ Add particle back-reaction
∙ Include disk self–gravity
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what’s next?
∙ Generate ALMA–like images (e.g. with RADMC-3D + CASA package)
∙ Extend integration time
∙ Add particle back-reaction
∙ Include disk self–gravity
∙ Different mass planets
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what’s next?
∙ Generate ALMA–like images (e.g. with RADMC-3D + CASA package)
∙ Extend integration time
∙ Add particle back-reaction
∙ Include disk self–gravity
∙ Different mass planets
∙ Relax isothermal approximation
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.conclusions
.
summary
∙ particle gaps are very prominent also for small mass planets
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summary
∙ particle gaps are very prominent also for small mass planets
∙ co-orbital particles with the inner planet are destabilized
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summary
∙ particle gaps are very prominent also for small mass planets
∙ co-orbital particles with the inner planet are destabilized
∙ particles in the ring clumps in few stable points
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.
summary
∙ particle gaps are very prominent also for small mass planets
∙ co-orbital particles with the inner planet are destabilized
∙ particles in the ring clumps in few stable points
∙ more massive the planets, wider the gap, narrower the ring, more
vortices
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.
summary
∙ particle gaps are very prominent also for small mass planets
∙ co-orbital particles with the inner planet are destabilized
∙ particles in the ring clumps in few stable points
∙ more massive the planets, wider the gap, narrower the ring, more
vortices
∙ ripples are observed for particles with high stopping time, orbiting
close to small mass planets
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summary
∙ the simulations with 1 thermal mass planets present wider rings
and narrow gaps, creating a similar dust distribution as observed
by the ALMA telescope
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summary
∙ the simulations with 1 thermal mass planets present wider rings
and narrow gaps, creating a similar dust distribution as observed
by the ALMA telescope
∙ if this is the case the gas emission from the same system is
expected to be much more smooth
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Questions?
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